Thanks to missions such as CoRoT and Kepler/K2, asteroseismology has demonstrated that it is a powerful tool to determine precise stellar parameters. Now, with the NASA TESS (Transiting Exoplanet Survey Satellite) mission, a new opportunity arose to use this technique on a sample of more than 20,000 bright main-sequence and subgiant stars. The standard light curves provided by the TESS Science Processing Operations Center (SPOC) are optimized for exoplanet search, the main goal of this mission, and could be improved to look for oscillations in solar-like stars. Our experience with Kepler have shown that the ideal apertures are larger than the standard ones. These apertures increase the signal-to-noise ratio (SNR) of the oscillation modes of the stars while improving the low-frequency stability of the light curve. We developed an automatic code to determine the optimal aperture to look for the oscillation modes for a large sample of solar-like stars, in particular, on planet host stars. Here we present the methodology and we will show examples of how we improve the SNR and detection of the modes using our apertures compared to other apertures obtained within the community.